adsabs/AstroCLIMB huggingface dataset:
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Top: HSA 100 μm map of Perseus E, convolved to 500 μm resolution and zero level corrected. Bottom: extrapolated 100 μm map from the HOTT thermal dust model.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Top: τ  HOTT of Perseus E. Bottom: T HOTT of Perseus E.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: Top left: the sky distribution of the LAEs within the CLAMATO field of view. Red circles and salmon triangles mark the position of pLAEs and sLAEs, respectively. The contours label the galaxy number density, and the dashed contour highlights the central overdensity. The background color map shows the projected Lyα forest fluctuations ﹩{\delta }_{F,2{\rm{D}}}^{{\rm{r}}{\rm{e}}{\rm{c}}}﹩ over redshift z = 2.40−2.54. Bottom left: histograms of ﹩{\delta }_{F,2{\rm{D}}}^{{\rm{r}}{\rm{e}}{\rm{c}}}﹩ of all LAEs (red steps), spectroscopic members of the Hyperion (green steps), and random galaxies (gray bars). The mean ﹩{\delta }_{F,2{\rm{D}}}^{{\rm{r}}{\rm{e}}{\rm{c}}}﹩ value of each sample is shown at the top axis. Bottom right: histograms of ﹩{\delta }_{F,3{\rm{D}}}^{{\rm{r}}{\rm{e}}{\rm{c}}}﹩ of the three galaxy samples. The mean ﹩{\delta }_{F,3{\rm{D}}}^{{\rm{r}}{\rm{e}}{\rm{c}}}﹩ value of each sample is marked at the top axis.
Paper: Evaluating Lyα Emission as a Tracer of the Largest Cosmic Structure at z ∼ 2.47
Authors: Yun Huang, Kyoung-Soo Lee, Olga Cucciati, Brian C. Lemaux, Marcin Sawicki, Nicola Malavasi, Vandana Ramakrishnan, Rui Xue, Letizia P. Cassara, Yi-Kuan Chiang, Arjun Dey, Stephen D. J. Gwyn, Nimish Hathi, Laura Pentericci, Moire K. M. Prescott, Gianni Zamorani
Figure caption: Sky positions of LAEs with X-ray (cyan circles), MIPS 24 μm (yellow stars), and VLA (white crosses) detection. The broad-line AGNs confirmed by spectroscopic surveys are shown as black dots. The smoothed LAE density map in the background and contours are identical to those shown in the top left panel of Figure 4.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Initial (left) and final (right) state of the single accretion torus 2.5D GRMHD numerical simulation. The mass density distribution in the meridional plane (x–z) is shown in blue. Color intensity corresponds to the values of the mass density, which is normalized to 1. Gray lines represent magnetic field lines. A weak magnetic field B ≐ 0.00033 (equivalent to β ≐ 5000) is initially in uniform configuration parallel to the z-axis. At the end of the simulation, when a relaxed state is reached, a split parabolic configuration can be found as a jet funnel (close to the z-axis), while the magnetic field is turbulent inside the accretion torus and corona. The black half circle is the BH horizon. All quantities here have geometrical units with M = 1. The mass density color bar has limited changes in interval from 0.3 to 1.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: “Two-corot” mass density distribution for double accretion tori rotating in the same direction. Color intensity corresponds to the values of the mass density (normalized to 1); blue has been used for the positive momenta ℓ > 0. Gray lines represent the weak magnetic field B ≐ 0.00033 corresponding to the initial plasma parameter β ≐ 5000 inside the inner torus center.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Time evolution of the mass density inside the double torus configuration “two-weak.” The inner torus (blue) has positive angular momentum, while the outer torus (red) has negative angular momentum; i.e., the tori are rotating in opposite directions. Color intensity corresponds to the values of the mass density (normalized ﹩{\rho }_{\max }=1﹩). Both tori have similar radial sizes, but the inner torus is more dense, making the influence of the outer torus on the accretion process negligible. All quantities here have geometrical units. For a detailed description, see also Figure 3.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Mass accretion rate for the single torus with initial uniform magnetic field. Several representative values of the magnetic field strength B have been used, distinguished by different colors. All quantities here have geometrical units (G = c = M = 1). Here and in all other places, the accretion rate (vertical axis) is calculated after the normalization of density (﹩\max (\rho =1)﹩). To transfer it to geometrical units, one should multiply the accretion rate by a factor ﹩{\rho }_{\max }﹩, the maximum (central) density of the torus, which is equivalent to 5.7 × 10−5 for this case.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Angular momentum and mass density radial profiles for double torus configurations. The blue curves refer to the inner torus, while the red refer to the outer torus. The torus center and inner and outer edges are shown by dashed lines. The Keplerian angular momentum profile is shown by the black curve. Logarithmic scale has been used on the horizontal axis. All quantities here have geometrical units (G = c = M = 1).
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Same as Figure 5, but this configuration (“two-strong”) has a very huge outer center rotation torus with the central density close to the inner torus’s density. Color intensity corresponds to the values of the normalized mass density. For a detailed description, see also Figure 3.
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Location and size of double torus structure components. Closed gray loops are mass density contours, with torus density and pressure maximum located at the torus center. The black circle is the central BH horizon. All quantities here have geometrical units (G = c = M = 1).
Paper: GRMHD Evolution of Interacting Double Accretion Tori Orbiting a Central Black Hole
Authors: Dilshodbek Bardiev, Martin Kološ, Daniela Pugliese, Zdeněk Stuchlík
Figure caption: Magnetic field intensity calculated for double corotating accretion disks, showing the existence of separation layer and toroidal plasmoids. Gray magnetic field lines are superimposed on the magnetic field intensity plot, where red (blue) represents regions with stronger (weaker) magnetic fields. The panels correspond to the bottom two panels of Figure 7; see time stamps in upper right corner.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: (a) Mean-subtracted activations using the 47-channel EfficientNetV2. The innermost planet has M = 0.28M  J , the second planet has M = 0.20M  J , the third planet has M = 0.36M  J , and the outermost planet has M = 0.02M  J . (b) Disk column density after an azimuthal rotation of ϕ = 131° and inclined by i = 36°. (c) Unconvolved velocity channel with the most obvious kink. (d) Corresponding convolved velocity channel. Based on the kink, the approximate location of the planet causing the most significant kink is in the white circle. The planets were correctly predicted with a confidence of >99%.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: (a) HD 97048 at 885 μm. (b) Δv = 0.96 km s−1 channel. Bottom: mean-subtracted activations from two different layers for HD 97048 using the 47-channel RegNet. The estimated planet location is given inside the white circle. The beams for the observations are given in the bottom right corner of panels (a) and (b).
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption:  p-values from testing the correlation between accuracy and the number of planets at different decision thresholds. The dashed black line is p = 0.05, which is the standard cutoff for statistical significance.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: Accuracy of all models for a given number of planets. Left: 50% decision threshold. Right: 95% decision threshold.
Paper: Locating Hidden Exoplanets in ALMA Data Using Machine Learning
Authors: J. P. Terry, C. Hall, S. Abreau, S. Gleyzer
Figure caption: (a) Typical example of mean-subtracted activations for a disk with no planet. (b) Disk column density after an azimuthal rotation of ϕ = 153° and inclined by i = 13°.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: Top: 21 cm line flux (S 21) vs. redshift for the NSA (purple) and UDG (red) samples. The nominal ALFALFA flux limit is shown by the dashed black line, while the minimum S 21 of the UDG sample is shown in red. The unfilled symbols show the expected S 21 of each of the galaxies in the UDG sample if we assume that the distribution over the H I fraction of the underlying UDG population is identical to that of NSA dwarfs. Bottom: the distribution over observed H I fractions for the NSA (filled purple histogram) and UDG (unfilled red histogram) samples. The hatched red histogram shows the distribution of H I fractions that we would expect to see from the UDG sample if the distribution over H I fractions is identical between the UDG population and NSA sample. We thus conclude that the UDG sample is inconsistent with having the same distribution over f H I as the NSA sample.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: Estimates of the SFR, stellar mass, and H I surface densities in a globally averaged sense, i.e., the ratio between the integrated measurement and the isophotal size of the galaxy. UDGs are shown in red and NSA dwarfs in purple for all cases. In this figure, we exclude all NSA dwarfs with stellar masses exceeding M ⋆ = 109 M ⊙.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison of the integrated properties of the samples derived in this work against the directly measured result of Leroy et al. (2008; beige points). In all panels, the red points show UDGs and the purple points show NSA dwarfs. From the left, we show the relationship between stellar mass and H I mass, the relationship between H I mass and SFR, and the SFMS. In the SFMS panel, we also show the results of the SDSS DR7 MPA-JHU value-added catalogs in grayscale (Kauffmann et al. 2003; Brinchmann et al. 2004; Salim et al. 2007). We find a good agreement between our results and those from the literature. Although UDGs have high H I masses for their stellar mass (left panel), they have relatively little SFR for their H I mass (middle panel).
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison between our estimates of the H I surface density radial profiles for the UDG (red solid curves) and NSA (purple solid curves) samples against spatially resolved H I measurements of dwarfs from the literature. We show the direct radial profiles of Leroy et al. (2008) in green, and Sérsic fits inferred for a sample of H I-rich UDGs from the H I spatial distribution metrics provided by Gault et al. (2021) in orange. We find that our radial profile estimates are in good agreement with these direct literature measurements.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Coverage of ALMA, Herschel/PACS, and MUSE data, marked with yellow dashed, red dashed–dotted, and cyan dotted lines, respectively, over a three-color HST image of M 104 appeared as Astronomy Picture of the Day on 2019 March 29. The HST data were obtained by the Hubble Heritage Team in the filters F435W (B), F555W (V), and F625W (r). (†Credits: ESA/Hubble & NASA/R. B. Andreo, https://apod.nasa.gov/apod/ap190329.html).
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Left: Plane-of-sky relative orientation angles of outflow pairs as a function of their projected separation distances. Middle: Plane-of-sky relative orientation angles of the local magnetic field directions at the positions of outflow pairs as a function of their projected separation distances. Right: 3D relative orientation angles of outflows pairs as a function of their projected separation distances. The data have been averaged in various separation distance bins, with the size of the circle indicating the number of samples in each distance bin (see legend). The gray dashed line illustrates 45◦ (left and middle panels) and 60◦ (right panel), which is expected from random relative orientations. The inset shows a zoom-in to the smallest scales from 0 to 4 pc.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Circular apertures selected for the detailed study of the different parts of the ring and the inner regions, plotted over the Hα and [C II] images in the top and bottom panels, respectively. The independent apertures uniformly sample the ring and are usually centered on star-forming knots. The aperture diameter corresponds to the [C II] beam. The circles are orange or green if the region is classified as H II or LIER according to the diagnostic diagrams (see Section 3.5).
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Integrated intensity, velocity, and FWHM maps of the CO, [C II], and Hα emission lines. Sky positions where lines have signal-to-noise ratios less than five are left black.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: Examples of spectra in three apertures. The CO, [C II], and Hα lines are shown in the top, middle, and lower panels, respectively. The orange line corresponds to the adopted fit.
Paper: A Molecular Gas Ring Hidden in the Sombrero Galaxy
Authors: Jessica Sutter, Dario Fadda
Figure caption: The ring of the Sombrero galaxy as seen from UV to submillimeter wavelengths. The PSF of each image is shown in the left bottom corner of each panel. The ellipse fitted to the ring is marked in black. NUV, Hα, and [C II] intensity images only have bright spots along the ring and weak continuous component.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption: Scatter plot between true f  v  and CASI-3D predicted f  v . The color indicates the normalized occurrence of the data point.
Paper: A Census of Outflow to Magnetic Field Orientations in Nearby Molecular Clouds
Authors: Duo Xu, Stella S. R. Offner, Robert Gutermuth, Jonathan C. Tan
Figure caption:  12CO emission of a synthetic outflow at two velocity channels (left column), the corresponding correction factor (middle column), and CASI-3D prediction (right column).
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Mean and variance of interpulsar correlations. We show results for an idealized GWB, a single CW source, and a realistic population-based GWB. We also show the theoretically expected mean and variance of the correlations under different assumptions. The small discrepancy between the theoretical and simulated CW curves is due to the anisotropic distribution of pulsars used for the simulation (see the Appendix). Note that we show the results in 20 angular bins, and the results were averaged over 100 realizations to reduce the scatter of these curves.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Number of binaries contributing 90% of the total strain in each frequency bin (N 90). We show this for the whole data set (purple) and for data sets with the top 1/10/100/1000 binaries removed (different shades of green). We also show the total number of binaries in each bin (N tot; gray histogram). Vertical dashed lines indicate frequencies where the total numbers of binaries reach 1000 and 100. Note that the lines for the data sets without the top 1000/100 asymptote to the corresponding vertical lines, indicating frequency bins where we remove a large fraction of the binaries.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Angular distribution of the characteristic amplitude in the frequency bin with 66.5 nHz < f obs < 68.7 nHz. We show sky maps for all binaries (first row) and with 1/10/100 brightest binaries removed (second/third/fourth rows). The left column shows the raw maps, while the right column shows the maps reconstructed with the same range of angular scales as was used for the anisotropy test (1 ≤ ℓ ≤ 6). Only the maps with 10 and 100 binaries removed passed the isotropy test in this example. The monopole term was subtracted from each map. Note the changing scale of the color maps, which we forced to be symmetric around 0.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Minimum number of sources removed to achieve statistical isotropy based on the κ  ℓ -test with ℓ between 1 and 6, N rem(1 ≤ ℓ ≤ 6). We show the median and 68% credible interval of N rem over 30 GWB realizations. We also show the number of binaries with an h  c  within a factor of 3 of the brightest binary in the frequency bin, N top(33.3%). Note how statistical isotropy is reached when N top(33.3%) ∼ 10. The black line shows the total number of sources in each frequency bin. The dashed (dotted) horizontal line shows the expected value of N rem due to the false negative (positive) probability of our test (see Table 1) if all maps are isotropic (anisotropic).
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Variance of the mean correlations over 100 realizations. We show results for an idealized GWB, a single CW source, and a realistic population-based GWB. Besides the same theoretical curves as in Figure 7, we also show the theoretical variance from cosmic variance only (Allen 2022). Note the different vertical scale compared to Figure 7.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Distribution of the median S/N over the sky for a particular source. Red stars indicate the locations of pulsars in our array (based on the NANOGrav 12.5 yr data set; see Alam et al. 2021), with their sizes corresponding to their sensitivity as defined in Equation (17). The black cross indicates the sky pixel with the highest median S/N.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Characteristic strain spectrum for all binaries (purple) and for various numbers of the brightest binaries removed (different shades of green). We also show a power-law spectrum for reference (dashed gray line).
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: Histogram of deviations from the HD curve for all three simulations we performed. The bottom panel shows the mean and 90% credible interval for the distribution of all individual correlation values. The top panel shows the distribution of mean correlation values calculated in each angular bin and each realization.
Paper: Exploring Realistic Nanohertz Gravitational-wave Backgrounds
Authors: Bence Bécsy, Neil J. Cornish, Luke Zoltan Kelley
Figure caption: GWB spectrum in a particular realization (blue histogram) and the brightest binary in each bin (blue circles). The binary we focus our attention on is indicated by the orange circle.
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Photons classified by their escaping places from the system. “A”: seed photons that directly leave the accretion cavity without any interaction. “B”: scattered photons that escape the system from the wall of the cavity. “C”: scattered photons that pass through the top/bottom surfaces of the outflow. “D”: scattered photons that leave the system from the side surface of the outflow. “E”: photons that escape from the wall of the cavity and entered into the AC.
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: The combination of thermal motion and bulk motion of the electrons. The left two panels show the probability density distribution functions of the velocity of electrons N(β), with bulk velocity v = 0.1c and v = 0.5c respectively. The right two panels show the relationship between the direction of motion of an electron and the velocity of the electron with v = 0.1c and v = 0.5c, respectively, in which α is the angle between the axis of the cavity and the direction of motion of the electron.
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Schematic illustration of the simulated geometry. The AC of the NS emits seed photons at the center of the accretion cavity, surrounded by an axially symmetric outflow.